As mentioned before, theoretical simulations predict an increase of the dust temperature with redshift, which is generally explained by several factors such as stronger radiation fields, lower dust masses, and more compact dust-emitting regions at high redshifts. Empirically, an increase of dust temperature with redshift has also been observed, e.g., by [1]}, though we note that this is still somewhat controversial as it could be a result of selection effects: since there is a positive correlation between dust temperature and dust luminosity, and flux-limited samples detecting higher luminosity sources at higher redshifts (e.g., [2]}). In fact, the direct temperature measurements of sources at \(z\gtrsim 6\)  with multi-band ALMA observations described above [3]}, [4]} do not follow the extrapolation of the temperature-redshift relation of [1]}: their temperatures are about 10 to 20 K lower than predicted by that relation. If these temperatures are typical for high-redshift galaxies, then the dust temperatures might not be high enough to reconcile the IR excesses with Milky Way-like dust attenuation in the IRX-\(\beta \)  relation, which would indicate that indeed galaxies at the EoR have different dust properties. However, it is to be expected that there is a spread in dust temperatures at any given redshift (depending on different galaxy properties), so larger samples of galaxies t \(z\gtrsim 6\)  with ALMA continuum observations are needed. One such samples comes from the REBELS survey described below.
